\section{Summary}\label{Sec. Summary}

    \numsou Planck cold clumps were mapped, \numsoutmc are in TMC, \numsoucmc in CMC and \numsoupmc are in PMC. In the \numvelcomp velocity components, \numcore cores are found in \numcompofcores clumps, \numcoretmc cores are in TMC, \numcorecmc in CMC and \numcorepmc are in PMC.

    \begin{enumerate}
      \item For all the \numsou clumps, \coaa and \cobb emissions were detected, while for \numcocc of them, \cocc emissions were detected. The average $T_{12}$ of cores in TMC is 3.8 K, and it is 3.7 K in CMC, 5.1 K in Perseus. Some spectra exhibit very low $T_{12}/T_{13}$ ratio.
          $T_{13}$ average at 1.9 K for cores in TMC and for California, mean $T_{13}$ is 1.8 K. While for Perseus, the cores in it are of $T_{13}$ average at 3.4 K. About half of the cores are of spectra with non-gaussian profiles.
          Physical parameters: excitation temperature, column density, velocity dispersion, LTE mass, virial mass and Jeans mass were calculated.
          

    \item We calculated the ratio of CO column density (from our observation) and H$_2$ column density (from Planck ECC data) and acquired the spatial distribution of CO abundance in TMC, CMC and PMC area. For the coherence of temperature between gas and dust, we found that 
        61\% cores have dust temperatures higher than gas temperatures. The $T_D/T_k$ is of average value 1.3$\pm$0.4. It is consistent with Goldreich- Kwan picture.

    \item From the statistical study of velocity dispersions and column density in the complex scale we found that
            for both of TMC and CMC,  cores are found with \sigmant generally larger than \sigmath, which indicate that non-thermal motions (turbulence) contributes more than thermal components supporting the cores. 

      \item In TMC and CMC, most of the cores are with $M_{vir}$ and $M_J$ larger than $M_{LTE}$, which suggest that the cores are probably without gravitational collapsing and not forming stars, and are not bound either. In CMC, we found 3 cores that have $M_J>M_{LTE}$ have spectra of non-gaussian profile.

      \item Associate objects for our mapped clumps are investigated. Among the \numsoucmc clumps in CMC 2 are found with X-ray object(s), 6 with radio, H I or Maser sources, 9  with IR objects, only 1 with HH object. From the CMC survey by \citep{2013ApJ...764..133H}, we found only 4 clumps are associated with YSO which indicate the low activity of star formation.
          
          Among the 37 clumps in TMC, 13 are found associated with X-ray source, 14 are found with radio, H I or Maser, 16 are found with IR objects. HH objects are found in 8 of them. 28 clumps are covered by IRAC/MIPS observation, but only in 8 of them YSO are found.
          Perseus is much more active and abundant of associated objects: Among the 10 clumps in it, 2 of them are with x-ray sources, while 7 of them are radio, H I or Maser sources. 8  are found with IR objects and 7 with HH objects. YSO are found in 5 of them.

    \end{enumerate}

\section*{Acknowledgment}
\begin{acknowledgements}
We are grateful for the assistance provided by staff of Qinghai Station of PMO during
the observation.
Thanks for the Key Laboratory for Radio Astronomy, CAS for partly support the telescope operating.
Thanks also to the anonymous referee, who have given us much constructive advice and illumination.
This work was partly supported by China Ministry of Science and Technology under State Key Development Program for Basic Research
(2012CB821800).
\end{acknowledgements}
